A preliminary study of the locking of an interferometer for gravitational wave detection

Caron, Bernard; Dominjon, A.; Drezen, C.; Flaminio, R.; Grave, X.; Hermel, R.; Marion, F.; Massonnet, L.; Mehmel, C.; Morand, R.; Mours, B.; Sannibale, V.; Yvert, M.

doi:10.1016/s0927-6505(96)00057-6

Cited by 18 publications

(18 citation statements)

References 4 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Indirect evidence for the existence of gravitational waves was provided by the orbital decay of the Hulse-Taylor pulsar (Hulse & Taylor 1975;Taylor & Weisberg 1989) and later with stronger constraints by the double pulsar (Burgay et al 2003;Lyne et al 2004). Direct detection of the gravitational wave signal of the inspiral of NS-NS, BH-NS, or BH-BH binaries and the subsequent merger and ring-down is expected to happen in the next few years, now that the advanced ground-based gravitational wave detectors aLIGO and Virgo are coming online (Caron et al 1997;Abbott et al 2009). …”

Section: Introductionmentioning

confidence: 99%

Merger Rates of Double Neutron Stars and Stellar Origin Black Holes: The Impact of Initial Conditions on Binary Evolution Predictions

Mink

Belczyński

2015

ApJ

197

151

View full text Add to dashboard Cite

The initial mass function (IMF), binary fraction, and distributions of binary parameters (mass ratios, separations, and eccentricities) are indispensable inputs for simulations of stellar populations. It is often claimed that these are poorly constrained, significantly affecting evolutionary predictions. Recently, dedicated observing campaigns have provided new constraints on the initial conditions for massive stars. Findings include a larger close binary fraction and a stronger preference for very tight systems. We investigate the impact on the predicted merger rates of neutron stars and black holes. Despite the changes with previous assumptions, we only find an increase of less than a factor of 2 (insignificant compared with evolutionary uncertainties of typically a factor of 10-100). We further show that the uncertainties in the new initial binary properties do not significantly affect (within a factor of 2) our predictions of double compact object merger rates. An exception is the uncertainty in IMF (variations by a factor of 6 up and down). No significant changes in the distributions of final component masses, mass ratios, chirp masses, and delay times are found. We conclude that the predictions are, for practical purposes, robust against uncertainties in the initial conditions concerning binary parameters, with the exception of the IMF. This eliminates an important layer of the many uncertain assumptions affecting the predictions of merger detection rates with the gravitational wave detectors aLIGO/aVirgo.

show abstract

Section: Introductionmentioning

confidence: 99%

Merger Rates of Double Neutron Stars and Stellar Origin Black Holes: The Impact of Initial Conditions on Binary Evolution Predictions

Mink

Belczyński

2015

ApJ

197

151

View full text Add to dashboard Cite

show abstract

“…As the search for Gravitational Waves is about to enter its golden age, with advanced LIGO [1], VIRGO [2], GEO 600 [3], TAMA 300 [4], as well as many other interferometers and CMB probes such as the South Pole Telescope [5] or Planck [6] for the detection of primordial Gravitational Waves, the time is right to reflect on what can be expected from a purely theoretical perspective. Even though General Relativity (GR) predicts the propagation of two polarizations, which have been indirectly tested with an unchallenged accuracy via binary pulsars timing delay, the presence of additional polarizations might not necessarily be ruled out, neither from a theoretical nor from an observational point of view.…”

Section: Introductionmentioning

confidence: 99%

Massive gravity on de Sitter and unique candidate for partially massless gravity

Rham

Renaux‐Petel

2013

J. Cosmol. Astropart. Phys.

129

View full text Add to dashboard Cite

Abstract. We derive the decoupling limit of Massive Gravity on de Sitter in an arbitrary number of space-time dimensions d. By embedding d-dimensional de Sitter into d + 1-dimensional Minkowski, we extract the physical helicity-1 and helicity-0 polarizations of the graviton. The resulting decoupling theory is similar to that obtained around Minkowski. We take great care at exploring the partially massless limit and define the unique fully non-linear candidate theory that is free of the helicity-0 mode in the decoupling limit, and which therefore propagates only four degrees of freedom in four dimensions. In the latter situation, we show that a new Vainshtein mechanism is at work in the limit m 2 → 2H 2 which decouples the helicity-0 mode when the parameters are different from that of partially massless gravity. As a result, there is no discontinuity between massive gravity and its partially massless limit, just in the same way as there is no discontinuity in the massless limit of massive gravity. The usual bounds on the graviton mass could therefore equivalently well be interpreted as bounds on m 2 − 2H 2 . When dealing with the exact partially massless parameters, on the other hand, the symmetry at m 2 = 2H 2 imposes a specific constraint on matter. As a result the helicity-0 mode decouples without even the need of any Vainshtein mechanism.

show abstract

“…We prescribe this evolution through the perturbative algorithm described below Eq. (12). The ppE corrected energy and angular momentum flux are given in Eqs.…”

Section: B Mapping Between Tilesmentioning

confidence: 99%

“…Fortunately, the next generation of ground based GW detectors-LIGO [5][6][7][8], KA-GRA [9,10], VIRGO [11][12][13], GEO [14][15][16][17]-are expected to soon observe binary black hole, binary neutron star, and black hole-neutron star mergers; the final stages of these collisions are expected to reach ∼ 10 −2 L p . Compact object binaries that have large orbital eccentricity, while emitting GWs in the frequency band of ground-based detectors, have long been dismissed as likely sources.…”

Section: Introductionmentioning

confidence: 99%

Parametrized post-Einsteinian framework for gravitational wave bursts

2014

View full text Add to dashboard Cite

In [1], we developed a parameterized post-Einsteinian (ppE) model for the evolution of gravitational wave (GW) bursts from highly eccentric binary systems in time-frequency space. We here correct a few mistakes in some ingredients of the model. I. KEPLER PROBLEM IN THE PPE FORMALISMAs part of the computation of a ppE burst model, we considered an effective one body description for binary systems with generic modifications to the Newtonian potential. We claimed that the Newtonian potential within a generic modified theory of gravity can be written as shown in Eq. (B1) of [1], where the corrections scale as M/r p , with M the total mass of the binary and r p the pericenter distance of the binary. While the derivations in Appendix B of [1] are self-consistent, this scaling of the corrections is not suitable for some modified theories. We here generalize the results of this appendix to allow the model to apply to a wider set of theories.For equatorial orbits, the corrections to the Newtonian kinetic energy and gravitational potential within a modified theory of gravity may be written aswhere µ is the reduce mass of the binary, (α,β,γ) are amplitude parameters that depend on the coupling constants of the theory, and (ã,b,c) ∈ R that control the post-Newtonian (PN With this potential, we now compute the corrections to orbital quantities necessary to construct the ppE burst model, namely the orbital energy, angular momentum, period, and pericenter velocity. Let us begin by considering the Lagrangian for the binary within an effective one-body formalism. At leading (Newtonian) PN order, the Lagrangian for equatorial orbits may be written as L = T − U , with T = (1/2)µ(ṙ 2 + r 2φ2 ) + δT and U = −µM/r + δU . This Lagrangian admits two conserved quantities associated with the orbital energy and angular momentum, specificallyBy studying the turning points (ṙ = 0) of Eq. (3), and writing E = E N + δE and L = L N + δL, we findwith the Newtonian energy and angular momentum (E N , L N ) given in Eqs. (5.2) and (5.3) in [2], andThese deformations can be related to the generic deformation for the energy and angular momentum given in nonlinearity of the point particle Lagrangian, higher order terms in the velocity can couple to the modifications to the metric. Here, we are only concerned with the leading order terms, i.e. those that scale as v 2 × (α,β,γ). arXiv:1404.0092v3 [gr-qc] 2 Oct 20172 Eqs. (27) and (28) where LO stands for the leading-order term in a PN expansion. Now, let us consider the orbital period within our ppE formalism. In order to do this, it is useful to parametrize the radius of the orbit aswhere p = r p (1 + e) is the semi-latus rectum of the orbit and ψ increases monotonically by 2π from one pericenter passage to the next. The reason for this parametrization is that, in general, any deformation to the Newtonian potential will cause the orbits to precess [3], and as a result, the orbit will return to pericenter when φ = 2π + O (M/r p ). Using ψ to parameterize the orbit allows us to avoid complications from ...

show abstract

A preliminary study of the locking of an interferometer for gravitational wave detection

Cited by 18 publications

References 4 publications

Merger Rates of Double Neutron Stars and Stellar Origin Black Holes: The Impact of Initial Conditions on Binary Evolution Predictions

Merger Rates of Double Neutron Stars and Stellar Origin Black Holes: The Impact of Initial Conditions on Binary Evolution Predictions

Massive gravity on de Sitter and unique candidate for partially massless gravity

Parametrized post-Einsteinian framework for gravitational wave bursts

Contact Info

Product

Resources

About